分类： 天文学 >> 天文学 提交时间： 2023-02-19
Le Ngoc Tram
Lars Bonne
Yue Hu
Enrique Lopez-Rodriguez
Jordan A. Guerra
Pierre Lesaffre
Antoine Gusdorf
Thiem Hoang
Min-Young Lee
Alex Lazarian
B-G Andersson
Simon Coude
Archana Soam
William D. Vacca
Hyeseung Lee
Michael Gordon
摘要： The heart of the Large Magellanic Cloud, 30 Doradus, is a complex region with a clear core-halo structure. Feedback from the stellar cluster R$\,$136 has been shown to be the main source of energy creating multiple pc-scale expanding-shells in the outer region, and carving a nebula core in the proximity of the ionization source. We present the morphology and strength of the magnetic fields (B-fields) of 30 Doradus inferred from the far-infrared polarimetric observations by SOFIA/HAWC+ at 89, 154, and 214$\,\mu$m. The B-field morphology is complex, showing bending structures around R$\,$136. In addition, we use high spectral and angular resolution [\textsc{CII}] observations from SOFIA/GREAT and CO(2-1) from APEX. The kinematic structure of the region correlates with the B-field morphology and shows evidence of multiple expanding shells. Our B-field strength maps, estimated using the Davis-Chandrasekhar-Fermi method and structure-function, show variations across the cloud within a maximum of 600, 450, and 350$\,\mu$G at 89, 154, and 214$\,\mu$m, respectively. We estimated that the majority of the 30 Doradus clouds are sub-critical and sub-Alfv\'enic. The probability distribution function of the gas density shows that the turbulence is mainly compressively driven, while the plasma beta parameter indicates supersonic turbulence. We show that the B-field is sufficient to hold the cloud structure integrity under feedback from R$\,$136. We suggest that supersonic compressive turbulence enables the local gravitational collapse and triggers a new generation of stars to form. The velocity gradient technique (VGT) using [\textsc{CII}] and CO(2-1) is likely to confirm these results.
分类： 天文学 >> 天文学 提交时间： 2023-02-19
Sam Geen
Poojan Agrawal
Paul A. Crowther
B. W. Keller
Alex de Koter
Zsolt Keszthelyi
Freeke van de Voort
Ahmad A. Ali
Frank Backs
Lars Bonne
Vittoria Brugaletta
Annelotte Derkink
Sylvia Ekström
Yvonne A. Fichtner
Luca Grassitelli
Ylva Götberg
Erin R. Higgins
Eva Laplace
Kong You Liow
Marta Lorenzo
摘要： Stars strongly impact their environment, and shape structures on all scales throughout the universe, in a process known as ``feedback''. Due to the complexity of both stellar evolution and the physics of larger astrophysical structures, there remain many unanswered questions about how feedback operates, and what we can learn about stars by studying their imprint on the wider universe. In this white paper, we summarize discussions from the Lorentz Center meeting `Bringing Stellar Evolution and Feedback Together' in April 2022, and identify key areas where further dialogue can bring about radical changes in how we view the relationship between stars and the universe they live in.
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